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{{refimprove|date=January 2016}}
{{Starbox begin
{{Starbox begin
| name=μ Columbae
| name=μ Columbae
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{{Starbox observe
{{Starbox observe
| epoch=J2000
| epoch=J2000
| ra=05<sup>h</sup> 45<sup>m</sup> 59.9<sup>s</sup>
| ra={{RA|05|45|59.89496}}<ref name=hipparcos/>
| dec={{DEC|&minus;32|18|23.1630}}<ref name=hipparcos/>
| dec=-32° 18&prime; 23&Prime;
| appmag_v=5.18<ref name=ducati>{{cite journal|bibcode=2002yCat.2237....0D|title=VizieR Online Data Catalog: Catalogue of Stellar Photometry in Johnson's 11-color system|journal=CDS/ADC Collection of Electronic Catalogues|volume=2237|author1=Ducati|first1=J. R.|year=2002}}</ref>
| appmag_v=5.15
| constell=[[Columba (constellation)|Columba]]
| constell=[[Columba (constellation)|Columba]]
}}
}}
{{Starbox character
{{Starbox character
| class=O9.5 V<ref name=gosss>{{cite journal|bibcode=2014ApJS..211...10S|title=The Galactic O-Star Spectroscopic Survey (GOSSS). II. Bright Southern Stars|journal=The Astrophysical Journal Supplement|volume=211|pages=10|author1=Sota|first1=A.|last2=Maíz Apellániz|first2=J.|last3=Morrell|first3=N. I.|last4=Barbá|first4=R. H.|last5=Walborn|first5=N. R.|last6=Gamen|first6=R. C.|last7=Arias|first7=J. I.|last8=Alfaro|first8=E. J.|year=2014|doi=10.1088/0067-0049/211/1/10}}</ref>
| class=O9.5 V
| b-v=-0.28
| b-v=&minus;0.28<ref name=ducati/>
| u-b=-1.06
| u-b=&minus;1.06<ref name=ducati/>
| variable=Suspected<ref name=gcvs>{{cite journal|bibcode=2009yCat....102025S|title=VizieR Online Data Catalog: General Catalogue of Variable Stars (Samus+ 2007-2013)|journal=VizieR On-line Data Catalog: B/gcvs. Originally published in: 2009yCat....102025S|volume=1|display-authors=etal|author1=Samus|first1=N. N.|last2=Durlevich|first2=O. V.|year=2009}}</ref>
| variable=Suspected
}}
}}
{{Starbox astrometry
{{Starbox astrometry
| radial_v=+109.00 ± 1.8<ref>{{cite journal|bibcode=2006AstL...32..759G|title=Pulkovo Compilation of Radial Velocities for 35 495 Hipparcos stars in a common system|journal=Astronomy Letters|volume=32|issue=11|pages=759|author1=Gontcharov|first1=G. A.|year=2006|doi=10.1134/S1063773706110065}}</ref>
| radial_v=+109.2
| prop_mo_ra=3.01
| prop_mo_ra=2.98<ref name=hipparcos/>
| prop_mo_dec=-22.62
| prop_mo_dec=&minus;22.24<ref name=hipparcos/>
| parallax=2.52
| parallax=2.52
| p_error=0.55
| p_error=0.55
| parallax_footnote=<ref name=hipparcos>{{cite journal|bibcode=2007A&A...474..653V|title=Validation of the new Hipparcos reduction|journal=Astronomy and Astrophysics|volume=474|issue=2|pages=653|author1=Van Leeuwen|first1=F.|year=2007|doi=10.1051/0004-6361:20078357}}</ref>
| dist_ly=1300
| dist_pc=400
| dist_ly=
| dist_pc=
| absmag_v=-2.84
| absmag_v=&minus;3.64<ref name=martins/>
}}
}}
{{Starbox detail
{{Starbox detail
| source=<ref name=martins>{{cite journal|bibcode=2005A&A...441..735M|arxiv=astro-ph/0507278|title=On stars with weak winds: The Galactic case|journal=Astronomy and Astrophysics|volume=441|issue=2|pages=735|author1=Martins|first1=F.|last2=Schaerer|first2=D.|last3=Hillier|first3=D. J.|last4=Meynadier|first4=F.|last5=Heydari-Malayeri|first5=M.|last6=Walborn|first6=N. R.|year=2005|doi=10.1051/0004-6361:20052927}}</ref>
| mass=12-15
| radius=4.5
| mass=16
| radius=6.58
| luminosity=23,300
| temperature=33,700
| luminosity=45,700
| temperature=33,000
⚫
| metal=?
| gravity=4.0
| rotation=1.5 days (~153 km/s.)
⚫
| metal=
| age=2.7 &times; 10<sup>6</sup>
| rotation=
| rotational_velocity=111
| age_myr=2 - 4
}}
}}
{{Starbox catalog
{{Starbox catalog
| names=[[Harvard Revised catalogue|HR]] 1996, [[Cordoba Durchmusterung|CD]] -32°2538, [[Henry Draper catalogue|HD]] 38666, [[Smithsonian Astrophysical Observatory Star Catalog|SAO]] 196149, [[Hipparcos catalogue|HIP]] 27204
| names=[[Harvard Revised catalogue|HR]]&nbsp;1996, [[Cordoba Durchmusterung|CD]]&minus;32°2538, [[Henry Draper catalogue|HD]]&nbsp;38666, [[Smithsonian Astrophysical Observatory Star Catalog|SAO]]&nbsp;196149, [[Hipparcos catalogue|HIP]]&nbsp;27204
}}
}}
{{Starbox end}}
{{Starbox end}}
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This is a relatively fast rotating star that completes a full revolution approximately every 1.5 days. (Compare this to our [[Sun]], which at only 22% of this star's diameter rotates only once every 25.4 days.) This rate of rotation is fairly typical for stars of this class.
This is a relatively fast rotating star that completes a full revolution approximately every 1.5 days. (Compare this to our [[Sun]], which at only 22% of this star's diameter rotates only once every 25.4 days.) This rate of rotation is fairly typical for stars of this class.


Based on measurements of [[proper motion]] and [[radial velocity]], astronomers know that this star and [[AE Aurigae]] are moving away from each other at a [[relative velocity]] of over 200&nbsp;km/s. Their common point of origin intersects with [[Iota Orionis]] in the [[Trapezium (astronomy)|Trapezium cluster]], some two and half million years in the past. The most likely scenario that could have created these [[runaway star]]s is a collision between two [[binary star]] systems, with the stars being ejected along different trajectories radial to the point of intersection.
Based on measurements of [[proper motion]] and [[radial velocity]], astronomers know that this star and [[AE Aurigae]] are moving away from each other at a [[relative velocity]] of over 200&nbsp;km/s. Their common point of origin intersects with [[Iota Orionis]] in the [[Trapezium (astronomy)|Trapezium cluster]], some two and half million years in the past. The most likely scenario that could have created these [[runaway star]]s is a collision between two [[binary star]] systems, with the stars being ejected along different trajectories radial to the point of intersection.<ref name=gualandris>{{cite journal|bibcode=2004MNRAS.350..615G|title=N-body simulations of stars escaping from the Orion nebula|journal=Monthly Notices of the Royal Astronomical Society|volume=350|issue=2|pages=615|author1=Gualandris|first1=Alessia|last2=Portegies Zwart|first2=Simon|last3=Eggleton|first3=Peter P.|year=2004|doi=10.1111/j.1365-2966.2004.07673.x}}</ref>


==Etymology==
==Etymology==

In [[Chinese astronomy]], Mu Columbae is called 屎, [[Pinyin]]: Shǐ, meaning '' Excrement'', because this star is marking itself and stand alone in ''Excrement'' asterism, [[Three Stars (Chinese constellation)|Three Stars]] mansion (see : [[Chinese constellation]]).<ref>{{zh icon}} [http://aeea.nmns.edu.tw/2006/0607/ap060715.html AEEA (Activities of Exhibition and Education in Astronomy) 天文教育資訊網 2006 年 7 月 15 日]</ref> 屎 (Shǐ) westernized into '''She''' by R.H. Allen, with the meaning is "the Secretions" <ref>[http://penelope.uchicago.edu/Thayer/E/Gazetteer/Topics/astronomy/_Texts/secondary/ALLSTA/Columba_Noae*.html Richard Hinckley Allen: Star Names — Their Lore and Meaning: Columbae]</ref>
In [[Chinese astronomy]], Mu Columbae is called 屎, [[Pinyin]]: Shǐ, meaning '' Excrement'', because this star is marking itself and stand alone in ''Excrement'' asterism, [[Three Stars (Chinese constellation)|Three Stars]] mansion (see : [[Chinese constellation]]).<ref>{{zh icon}} [http://aeea.nmns.edu.tw/2006/0607/ap060715.html AEEA (Activities of Exhibition and Education in Astronomy) 天文教育資訊網 2006 年 7 月 15 日]</ref> 屎 (Shǐ) westernized into '''She''' by R.H. Allen, with the meaning is "the Secretions" <ref>[http://penelope.uchicago.edu/Thayer/E/Gazetteer/Topics/astronomy/_Texts/secondary/ALLSTA/Columba_Noae*.html Richard Hinckley Allen: Star Names — Their Lore and Meaning: Columbae]</ref>


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==References==
==References==
* A. Blaauw & W.W. Morgan, 1954, "The Space Motions of AE Aurigae and mu Columbae with Respect to the Orion Nebula", ''Astrophysical Journal'', v.119, p.&nbsp;625.
* R. Hoogerwerf, J.H.J. de Bruijne, P.T. de Zeeuw, 2000, "The origin of runaway stars", ''Astrophysical Journal'', v.544, issue 2, pp.&nbsp;L133-L136.
{{reflist}}
{{reflist}}


==External links==
==Further reading==
* {{cite journal|bibcode=1954ApJ...119..625B|title=The Space Motions of AE Aurigae and μ Columbae with Respect to the Orion Nebula|journal=Astrophysical Journal|volume=119|pages=625|author1=Blaauw|first1=A.|last2=Morgan|first2=W. W.|year=1954|doi=10.1086/145866}}
* [http://www.astro.uiuc.edu/~kaler/sow/mucol.html Mu Columbae] by Professor Jim Kaler.
* {{cite journal|bibcode=2001A&A...365...49H|arxiv=astro-ph/0010057|title=On the origin of the O and B-type stars with high velocities. II. Runaway stars and pulsars ejected from the nearby young stellar groups|journal=Astronomy and Astrophysics|volume=365|issue=2|pages=49|author1=Hoogerwerf|first1=R.|last2=De Bruijne|first2=J. H. J.|last3=De Zeeuw|first3=P. T.|year=2001|doi=10.1051/0004-6361:20000014}}

{{Stars of Columba}}
{{Stars of Columba}}


Revision as of 20:12, 11 April 2016

μ Columbae
Location of μ Columbae (circled)
Observation data
Epoch J2000      Equinox J2000
Constellation Columba
Right ascension 05h 45m 59.89496s[1]
Declination −32° 18′ 23.1630″[1]
Apparent magnitude (V) 5.18[2]
Characteristics
Spectral type O9.5 V[3]
U−B color index −1.06[2]
B−V color index −0.28[2]
Variable type Suspected[4]
Astrometry
Radial velocity (Rv)+109.00 ± 1.8[5] km/s
Proper motion (μ) RA: 2.98[1] mas/yr
Dec.: −22.24[1] mas/yr
Parallax (π)2.52 ± 0.55 mas[1]
Distanceapprox. 1,300 ly
(approx. 400 pc)
Absolute magnitude (MV)−3.64[6]
Details[6]
Mass16 M☉
Radius6.58 R☉
Luminosity45,700 L☉
Surface gravity (log g)4.0 cgs
Temperature33,000 K
Rotational velocity (v sin i)111 km/s
Age2 - 4 Myr
Other designations
HR 1996, CD−32°2538, HD 38666, SAO 196149, HIP 27204

Mu Columbae (μ Col, μ Columbae) is a star in the constellation of Columba. It is one of the few O-class stars that are visible to the unaided eye. The star is known to lie approximately 1,300 light years from the Solar System (with an error margin of a few hundred light years).

This is a relatively fast rotating star that completes a full revolution approximately every 1.5 days. (Compare this to our Sun, which at only 22% of this star's diameter rotates only once every 25.4 days.) This rate of rotation is fairly typical for stars of this class.

Based on measurements of proper motion and radial velocity, astronomers know that this star and AE Aurigae are moving away from each other at a relative velocity of over 200 km/s. Their common point of origin intersects with Iota Orionis in the Trapezium cluster, some two and half million years in the past. The most likely scenario that could have created these runaway stars is a collision between two binary star systems, with the stars being ejected along different trajectories radial to the point of intersection.[7]

Etymology

In Chinese astronomy, Mu Columbae is called 屎, Pinyin: Shǐ, meaning Excrement, because this star is marking itself and stand alone in Excrement asterism, Three Stars mansion (see : Chinese constellation).[8] 屎 (Shǐ) westernized into She by R.H. Allen, with the meaning is "the Secretions" [9]

This star, along with ζ CMa, λ CMa, γ Col, δ Col, θ Col, κ Col, λ Col and ξ Col, were Al Ḳurūd (ألقرد - al-qird), the Apes.[10]

References

  1. ^ a b c d e Van Leeuwen, F. (2007). "Validation of the new Hipparcos reduction". Astronomy and Astrophysics. 474 (2): 653. Bibcode:2007A&A...474..653V. doi:10.1051/0004-6361:20078357.
  2. ^ a b c Ducati, J. R. (2002). "VizieR Online Data Catalog: Catalogue of Stellar Photometry in Johnson's 11-color system". CDS/ADC Collection of Electronic Catalogues. 2237. Bibcode:2002yCat.2237....0D.
  3. ^ Sota, A.; Maíz Apellániz, J.; Morrell, N. I.; Barbá, R. H.; Walborn, N. R.; Gamen, R. C.; Arias, J. I.; Alfaro, E. J. (2014). "The Galactic O-Star Spectroscopic Survey (GOSSS). II. Bright Southern Stars". The Astrophysical Journal Supplement. 211: 10. Bibcode:2014ApJS..211...10S. doi:10.1088/0067-0049/211/1/10.
  4. ^ Samus, N. N.; Durlevich, O. V.; et al. (2009). "VizieR Online Data Catalog: General Catalogue of Variable Stars (Samus+ 2007-2013)". VizieR On-line Data Catalog: B/gcvs. Originally published in: 2009yCat....102025S. 1. Bibcode:2009yCat....102025S.
  5. ^ Gontcharov, G. A. (2006). "Pulkovo Compilation of Radial Velocities for 35 495 Hipparcos stars in a common system". Astronomy Letters. 32 (11): 759. Bibcode:2006AstL...32..759G. doi:10.1134/S1063773706110065.
  6. ^ a b Martins, F.; Schaerer, D.; Hillier, D. J.; Meynadier, F.; Heydari-Malayeri, M.; Walborn, N. R. (2005). "On stars with weak winds: The Galactic case". Astronomy and Astrophysics. 441 (2): 735. arXiv:astro-ph/0507278. Bibcode:2005A&A...441..735M. doi:10.1051/0004-6361:20052927.
  7. ^ Gualandris, Alessia; Portegies Zwart, Simon; Eggleton, Peter P. (2004). "N-body simulations of stars escaping from the Orion nebula". Monthly Notices of the Royal Astronomical Society. 350 (2): 615. Bibcode:2004MNRAS.350..615G. doi:10.1111/j.1365-2966.2004.07673.x.
  8. ^ Template:Zh icon AEEA (Activities of Exhibition and Education in Astronomy) 天文教育資訊網 2006 年 7 月 15 日
  9. ^ Richard Hinckley Allen: Star Names — Their Lore and Meaning: Columbae
  10. ^ Davis Jr., G. A. (October 1944). "The Pronunciations, Derivations, and Meanings of a Selected List of Star Names". Popular Astronomy. 18: 14. Bibcode:1944PA.....52....8D.

Further reading

Retrieved from "https://en.wikipedia.org/w/index.php?title=Mu_Columbae&oldid=714779293"